Solar Electron Bursts Observed Below 1.4 keV by ACE and Genesis: Characteristics and Implications for Particle Transport

Details Solar Electron Bursts Observed Below 1.4 keV by ACE and Genesis: Characteristics and Implications for Particle Transport Solar Electron Bursts Observed Below 1.4 keV by ACE and Genesis: Characteristics and Implications for Particle Transport

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsh33a..03d&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SH33A-03

Physics

2118 Energetic Particles, Solar, 7514 Energetic Particles (2114), 7807 Charged Particle Motion And Acceleration, 7859 Transport Processes

Scientific paper

Solar active processes frequently produce electron bursts at energies below 1.4 keV. The characteristics of these solar electron bursts vary considerably from event to event due to the physical processes involved in their acceleration and propagation to Earth. Previous observations have shown that some bursts have a broader pitch-angle distribution than the preceding strahl distribution, suggesting that propagation effects are important for understanding 1 AU observations. We present a study of the pitch-angle distributions of suprathermal electrons observed by ACE and Genesis before, during, and after solar bursts. We report the fraction of burst beams that broaden, the conditions under which they broaden, and the energy dependence of the burst beam width. We find that most long duration, high intensity bursts broaden. We often find a delay in the onset of burst beam broadening relative to the burst onset. The fact that some bursts broaden relative to the preceding strahl suggests that broadening occurs by a self-generated process. The facts that high intensity bursts broaden preferentially and that broadening is delayed suggest that this process has a threshold level.

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